Euclid. Predicting scaling relations for emission-line galaxies using simulated data
Abstract
The Euclid spectroscopic surveys will substantially increase the number of observed emission-line galaxies. We assess the ability of the Euclid Wide Survey (EWS) and Euclid Deep Survey (EDS), at the final DR3 depth, to recover the star-forming main sequence (MS), dust-mass relation (DMR), and mass-metallicity relation (MZR) from emission-line measurements. We use MAMBO (mocks with abundance matching in Bologna) spectroscopic simulations processed with the official Euclid pipelines. The MS is traced over 0≤ z≤ 4 using Paβ, Hα, and [OII] as SFR tracers. The shallow EWS flux limit biases the MS towards higher normalisation and a flatter slope by selecting the brightest, most strongly star-forming galaxies. The deeper EDS enables almost complete sampling with Paβ and Hα at log10(M*/M⊙)≥10.3 over 0≤ z≤ 1.88, with mild biases at both redshift limits. The [OII]-based MS is increasingly biased towards higher SFRs at the highest redshifts. The DMR is traced through the Balmer decrement over 1.45≤ z≤ 1.88 and 0.9≤ z≤ 1.88 in the EWS and EDS, respectively. The derived colour excess agree well with the input values, although detecting the faint Hβ line restricts the sample to less obscured galaxies at fixed M*, particularly in the EWS; the DMR is better sampled in the EDS. Finally, a golden sample detected in multiple optical rest-frame emission lines at 1.49≤ z≤ 1.88 recovers gas-phase metallicities with typical accuracy of 0.1 dex at log10(M*/M⊙)≥10, while lower-mass galaxies show biases up to 0.15 dex. Relative to H-band limited sample, this sample preferentially traces the upper MS and lower MZR. Despite the simplified simulations lacking effects such as mutual spectral contamination and detector persistence, these forecasts provide a benchmark for future Euclid spectroscopic analyses.
Related
- From Scaling Relations to Physical Laws: Constraining the Physics of Star Formation Across Local Galaxies
- Understanding galaxies and the origin of the golden mass through the study of scaling relations across cosmic history
- Inflow-driven galaxy evolution - II: A hierarchy in the scaling relations of star-forming galaxies
- Evolution of the morphology-density and morphology-mass relations of quiescent galaxies at 0.5 {2}lt;z<$ 2.5 in the COSMOS-Web survey
- Infrared spectroscopy of gas-phase hydrogenated and methylated pyrenes: From laboratory spectra to the simulated 3.4 μm emission band
BibTeX
@misc{collaboration2026euclid,
title = {{Euclid. Predicting scaling relations for emission-line galaxies using simulated data}},
author = {Euclid Collaboration and C. Mancini and L. Gabarra and S. Quai and L. Pozzetti and P. Cassata and M. Talia and M. Scodeggio and M. Bolzonella and M. Moresco and D. Vergani and E. Maiorano and V. Le Brun and B. R. Granett and S. Bisogni and A. Gargiulo and G. Vietri and M. Siudek and R. Ragusa and G. Herzog and G. De Lucia and L. Scharré and M. Fumana and M. Hirschmann and V. Allevato and L. Bisigello and A. Enia and A. Feltre and G. Rodighiero and G. Zamorani and P. Corcho-Caballero and X. Lopez Lopez and S. Andreon and N. Auricchio and C. Baccigalupi and M. Baldi and A. Balestra and S. Bardelli and P. Battaglia and A. Biviano and E. Branchini and M. Brescia and S. Camera and V. Capobianco and C. Carbone and J. Carretero and M. Castellano and G. Castignani and S. Cavuoti and P. -Y. Chabaud and A. Cimatti and C. Colodro-Conde and G. Congedo and L. Conversi and Y. Copin and F. Courbin and H. M. Courtois and H. Degaudenzi and S. de la Torre and H. Dole},
howpublished = {arXiv},
year = {2026},
month = nov,
doi = {10.48550/arxiv.2611.05482},
eprint = {2611.05482},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2611.05482},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - Euclid. Predicting scaling relations for emission-line galaxies using simulated data
AU - Euclid Collaboration
AU - C. Mancini
AU - L. Gabarra
AU - S. Quai
AU - L. Pozzetti
AU - P. Cassata
AU - M. Talia
AU - M. Scodeggio
AU - M. Bolzonella
AU - M. Moresco
AU - D. Vergani
AU - E. Maiorano
AU - V. Le Brun
AU - B. R. Granett
AU - S. Bisogni
AU - A. Gargiulo
AU - G. Vietri
AU - M. Siudek
AU - R. Ragusa
AU - G. Herzog
AU - G. De Lucia
AU - L. Scharré
AU - M. Fumana
AU - M. Hirschmann
AU - V. Allevato
AU - L. Bisigello
AU - A. Enia
AU - A. Feltre
AU - G. Rodighiero
AU - G. Zamorani
AU - P. Corcho-Caballero
AU - X. Lopez Lopez
AU - S. Andreon
AU - N. Auricchio
AU - C. Baccigalupi
AU - M. Baldi
AU - A. Balestra
AU - S. Bardelli
AU - P. Battaglia
AU - A. Biviano
AU - E. Branchini
AU - M. Brescia
AU - S. Camera
AU - V. Capobianco
AU - C. Carbone
AU - J. Carretero
AU - M. Castellano
AU - G. Castignani
AU - S. Cavuoti
AU - P. -Y. Chabaud
AU - A. Cimatti
AU - C. Colodro-Conde
AU - G. Congedo
AU - L. Conversi
AU - Y. Copin
AU - F. Courbin
AU - H. M. Courtois
AU - H. Degaudenzi
AU - S. de la Torre
AU - H. Dole
PY - 2026
DA - 2026/11/03
PB - arXiv
DO - 10.48550/arxiv.2611.05482
UR - https://arxiv.org/abs/2611.05482
AB - The Euclid spectroscopic surveys will substantially increase the number of observed emission-line galaxies. We assess the ability of the Euclid Wide Survey (EWS) and Euclid Deep Survey (EDS), at the final DR3 depth, to recover the star-forming main sequence (MS), dust-mass relation (DMR), and mass-metallicity relation (MZR) from emission-line measurements. We use MAMBO (mocks with abundance matching in Bologna) spectroscopic simulations processed with the official Euclid pipelines. The MS is traced over 0≤ z≤ 4 using Paβ, Hα, and [OII] as SFR tracers. The shallow EWS flux limit biases the MS towards higher normalisation and a flatter slope by selecting the brightest, most strongly star-forming galaxies. The deeper EDS enables almost complete sampling with Paβ and Hα at log_10(M_*/M_⊙)≥10.3 over 0≤ z≤ 1.88, with mild biases at both redshift limits. The [OII]-based MS is increasingly biased towards higher SFRs at the highest redshifts. The DMR is traced through the Balmer decrement over 1.45≤ z≤ 1.88 and 0.9≤ z≤ 1.88 in the EWS and EDS, respectively. The derived colour excess agree well with the input values, although detecting the faint Hβ line restricts the sample to less obscured galaxies at fixed M_*, particularly in the EWS; the DMR is better sampled in the EDS. Finally, a golden sample detected in multiple optical rest-frame emission lines at 1.49≤ z≤ 1.88 recovers gas-phase metallicities with typical accuracy of 0.1 dex at log_10(M_*/M_⊙)≥10, while lower-mass galaxies show biases up to 0.15 dex. Relative to H-band limited sample, this sample preferentially traces the upper MS and lower MZR. Despite the simplified simulations lacking effects such as mutual spectral contamination and detector persistence, these forecasts provide a benchmark for future Euclid spectroscopic analyses.
ER -